A data-driven MHD model of the weakly-ionized chromosphere
A data-driven MHD model of the weakly-ionized chromosphere
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DOI：
10.1088/1742-6596/1620/1/012026
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发表时间：
2020-07
期刊：
影响因子：
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通讯作者：
Mehmet Sarp Yalim;A. Prasad;N. Pogorelov;G. Zank;Q. Hu
中科院分区：
文献类型：
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作者：
Mehmet Sarp Yalim;A. Prasad;N. Pogorelov;G. Zank;Q. Hu
从理论和模型的角度来看，太阳色球层的物理学是复杂的。从光球到日冕的等离子体温度从~ 5000 K增加到~ 100万K，距离色球层和过渡区仅为~ 10000 km。太阳大气的某些区域具有足够低的温度和电离率，可以被认为是弱电离的。特别是在较低的色球层，这是正确的。在本文中，我们概述了数据驱动的弱电离色球磁流体动力学模型，并给出了一个基准结果。它利用的是比库仑电阻率大几个数量级的整流电阻率。因此欧姆定律包括各向异性耗散。我们研究了在耀斑产生活动区（AR） 11166演化过程中，coling电阻率对色球层加热和磁重联的影响。特别地，我们分析了来自AR11166的C2.0耀斑，发现归一化重联率为0.12。
The physics of the solar chromosphere is complex from both theoretical and modeling perspectives. The plasma temperature from the photosphere to corona increases from ∼5, 000 K to ∼1 million K over a distance of only ∼10, 000 km from the chromosphere and the transition region. Certain regions of the solar atmosphere have sufficiently low temperature and ionization rates to be considered as weakly-ionized. In particular, this is true at the lower chromosphere. In this paper, we present an overview of our data-driven magnetohydrodynamics model for the weakly-ionized chromosphere and show a benchmark result. It utilizes the Cowling resistivity which is orders of magnitude greater than the Coulomb resistivity. Ohm’s law therefore includes anisotropic dissipation. We investigate the effects of the Cowling resistivity on heating and magnetic reconnection in the chromosphere as the flare-producing active region (AR) 11166 evolves. In particular, we analyze a C2.0 flare emerging from AR11166 and find a normalized reconnection rate of 0.12.